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Oxygen Abundance Distributions in Six Late-Type Galaxies Based  on SALT Spectra of H II Regions

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Oxygen Abundance Distributions in Six Late-Type Galaxies Based  on SALT Spectra of H II Regions A&A 582, A35 (2015) Astronomy DOI: 10.1051/0004-6361/201526311 & c ESO 2015 Astrophysics Oxygen abundance distributions in six late-type galaxies based on SALT spectra of H II regions I. A. Zinchenko1,2,A.Y.Kniazev3,4,5,E.K.Grebel1, and L. S. Pilyugin1,2,6 1 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12–14, 69120 Heidelberg, Germany e-mail: [email protected] 2 Main Astronomical Observatory, National Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho St., 03680 Kyiv, Ukraine 3 South African Astronomical Observatory, PO Box 9, 7935 Observatory, Cape Town, South Africa 4 Southern African Large Telescope Foundation, PO Box 9, 7935 Observatory, Cape Town, South Africa 5 Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskij Pr. 13, 119992 Moscow, Russia 6 Kazan Federal University, 18 Kremlyovskaya St., 420008 Kazan, Russian Federation Received 14 April 2015 / Accepted 4 August 2015 ABSTRACT Spectra of 34 H ii regions in the late-type galaxies NGC 1087, NGC 2967, NGC 3023, NGC 4030, NGC 4123, and NGC 4517A were observed with the South African Large Telescope (SALT). In all 34 H ii regions, oxygen abundances were determined through the “counterpart” method (C method). Additionally, in two H ii regions in which we detected auroral lines, we measured oxygen abundances with the classic Te method. We also estimated the abundances in our H ii regions using the O3N2 and N2 calibrations and compared those with the C-based abundances. With these data, we examined the radial abundance distributions in the disks of our target galaxies. We derived surface-brightness profiles and other characteristics of the disks (the surface brightness at the disk center and the disk scale length) in three photometric bands for each galaxy using publicly available photometric imaging data. The radial distributions of the oxygen abundances predicted by the relation between abundance and disk surface brightness in the W1band obtained for spiral galaxies in our previous study are close to the radial distributions of the oxygen abundances determined from the analysis of the emission line spectra for four galaxies where this relation is applicable. Hence, when the surface-brightness profile of a late-type galaxy is known, this parametric relation can be used to estimate the likely present-day oxygen abundance in the disk of the galaxy. Key words. galaxies: abundances – HII regions – galaxies: general 1. Introduction It should be emphasized that the C method produces abun- dances on the same metallicity scale as the Te-method. In con- Metallicities play a key role in studies of galaxies. The present- trast, metallicities derived using one of the many calibrations day abundance distributions across a galaxy provide important based on photoionization models tend to show large discrepan- information about the evolutionary status of that galaxy and form cies (of up to ∼0.6 dex) with respect to Te-based abundances the basis for the construction of models of the chemical evolution (see the reviews by Kewley & Ellison 2008; López-Sánchez of galaxies. & Esteban 2010; López-Sánchez et al. 2012). Coupling our Oxygen abundances and their gradients in the disks of late- emission-line measurements with available line measurements type galaxies are typically based on emission-line spectra of in- from the literature or public databases, we measured the radial dividual H ii regions. When the auroral line [O iii]λ4363 is de- distributions of the oxygen abundances across the disks of six tected in the spectrum of an H ii region, the Te-based oxygen galaxies. / (O H)Te abundance can be derived using the standard equations The study of the correlations between the oxygen abundance of the Te-method. In our current study, we do not always have and other properties of spiral and irregular galaxies is impor- this information and use alternative methods where the auroral tant for understanding the formation and evolution of galax- line is not detected. In those cases, we estimate the oxygen abun- ies. The correlation between the local oxygen abundance and dances from strong emission lines using a recently suggested the stellar surface brightness (the OH – SBrelation) or surface method (called the “C method”) for abundance determinations mass density has been a subject of discussion for a long time of Pilyugin et al. (2012)andPilyugin et al. (2014a). When the (Webster & Smith 1983; Edmunds & Pagel 1984; Vila-Costas & strong lines R3, N2,andS 2 are measured in the spectrum of an Edmunds 1992; Ryder 1995; Moran et al. 2012; Rosales-Ortega ii / H region, the oxygen (O H)CSN abundance can be determined. et al. 2012; Sánchez et al. 2014). We examined the relations be- When the strong lines R2, R3,andN2 are measured in the spec- tween the oxygen abundance and the disk surface brightness in / trum, we can measure the oxygen (O H)CON abundance. the infrared W1 band of the Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010)atdifferent fractions of the opti- Based on observations made with the Southern African Large cal isophotal radius R25 in our previous paper (Pilyugin et al. Telescope, programs 2012-1-RSA_OTH-001, 2012-2-RSA_OTH-003 2014b). We found evidence that the OH – SBrelation depends and 2013-1-RSA_OTH-005. on the galactocentric distance taken as a fraction of the optical Article published by EDP Sciences A35, page 1 of 14 A&A 582, A35 (2015) Fig. 1. SDSS images of our target galaxies with marked positions of the slits used in the present investigation. radius R25 and on other properties of a galaxy, namely its disk 2. Our galaxy sample scale length and the morphological T-type. In that study, we sug- gested a parametric OH – SBrelation for spiral galaxies. Our original sample of spiral galaxies for follow-up observations with the Southern African Large Telescope (SALT; Buckley In our current paper, we present results from observations et al. 2006; O’Donoghue et al. 2006) was devised based on Sloan of emission-line spectra of H ii regions in six spiral galaxies. Digital Sky Survey (SDSS) images and the fact that SALT can These observations were obtained with the South African Large observe targets with a declination δ<10 degrees and has a field Telescope as a part of our investigation of the abundance prop- of view of 8 arcmin. Each selected spiral galaxy contains a suf- erties of nearby late-type galaxies (Pilyugin et al. 2014a,b). ficiently large number of bright H ii regions distributed across the whole galaxy disk and fitting SALT’s field of view. The total We constructed radial surface-brightness profiles of our sample consists of ∼30 nearby galaxies that are located in the galaxies in the infrared W1 band using the photometric maps equatorial sky region. obtained by the WISE satellite (Wright et al. 2010). The char- Out of this sample of 58 galaxies, we have obtained spec- acteristics of the disk for each galaxy were obtained through tra of H ii regions in six galaxies (NGC 1087, NGC 2967, bulge-disk decomposition. The radial distributions of the oxygen NGC 3023, NGC 4030, NGC 4123, NGC 4517A) thus far. In abundances predicted by the parametric OH – SB relation are Fig. 1 we present the images and slit positions for those galax- compared to the radial distributions of the oxygen abundances ies. For a detailed description of the observations, we refer to determined from the analysis of the emission-line spectra of the Sect. 3. H ii regions in our target galaxies. Table 1 lists the general characteristics of each galaxy. The paper is organized as follows. Our sample of galaxies We listed the most widely used identifications for our target is presented in Sect. 2. The spectroscopic observations and data galaxies, i.e., the designations in the New General Catalogue reduction are described in Sect. 3. The photometric properties of (NGC) and in the Uppsala General Catalog of Galaxies (UGC). our galaxies are discussed in Sect. 4. The oxygen abundances are The morphological type of the galaxy and morphological type presented in Sect. 5. Section 6 contains a discussion and a brief code T were adopted from leda (Lyon-Meudon Extragalactic summary of the main results. Database; Paturel et al. 1989, 2003). The right ascension and declination were taken from the NASA/IPAC Extragalactic Throughout the paper, we use the following standard nota- Database (ned)1. The inclination of each galaxy, the position tions for the line intensities I: angle of the major axis, and the isophotal radius R25 in arcmin R = I[O III]λ4363/IHβ, = R2 I[O II]λ3727+λ3729/IHβ, 1 The NASA/IPAC Extragalactic Database (ned) is operated by the N2 = I[N II]λ6548+λ6584/IHβ, Jet Populsion Laboratory, California Institute of Technology, under con- S 2 = I[S II]λ6717+λ6731/IHβ, tract with the National Aeronautics and Space Administration. http:// R3 = I[O III]λ4959+λ5007/IHβ. ned.ipac.caltech.edu/ A35, page 2 of 14 I. A. Zinchenko et al.: Oxygen abundance distributions in six galaxies Table 1. Adopted and derived properties of our target galaxies. Name NGC 1087 NGC 2967 NGC 3023 NGC 4030 NGC 4123 NGC 4517A UGC 2245 UGC 5180 UGC 5269 UGC 6993 UGC 7116 UGC 7685 Morphological type, type code T SABc, 5.0 Sc, 5.2 SABc, 5.5 Sbc, 4.0 Sc, 5.0 SBdm, 8.0 Right ascension (J2000.0) [deg] 41.604852 145.513729 147.469112 180.098445 182.046296 188.117319 Declination (J2000.0) [deg] –0.498649 0.336438 0.618167 –1.100095 2.878283 0.389670 Inclination [deg], ellipticity 53.0, 0.39 21.6, 0.07 49.5, 0.35 36.9, 0.20 43.1, 0.27 50.2, 0.36 Position angle [deg] 1 151 86 38 128 23 a Isophotal radius R25 [arcmin] 1.86 1.33 1.02 1.89 1.69 1.40 Distance [Mpc] 20.1 29.5 29.4 26.4 27.3 27.8 Isophotal radius R25 [kpc] 10.86 11.41 8.72 14.51 13.42 11.32 Disk scale length in W1 band [kpc] 2.45 1.97 3.36 4.70 4.90 b −2 Logarithm of W1 brightness of disk center [L pc ] 3.056 3.315 3.234 2.557 1.955 Notes.
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